Background: A hip fracture may occur spontaneously prior to the hip impact, due to the muscle pulling force exceeding the strength of the femur. Objects: We conducted falling experiments with humans to measure the activity of the hip muscles, and to examine how this was affected by the fall type. Methods: Eighteen individuals fell and landed sideways on a mat, by mimicking video-captured real-life older adults’ falls. Falling trials were acquired with three fall directions: forward, backward, or sideways, and with three knee positions at the time of hip impact, where the landing side knee was free of constraint, or contacted the mat or the contralateral knee. During falls, the activities of the iliopsoas (Ilio), gluteus medius (Gmed), gluteus maximus (Gmax) and adductor longus (ADDL) muscles were recorded. Outcome variables included the time to onset, activity at the time of hip impact, and timing of the peak activity with respect to the time of hip impact. Results: For Ilio, Gmed, Gmax, and ADDL, respectively, EMG onset averaged 292, 304, 350, and 248 ms after fall initiation. Timing of the peak activity averaged 106, 96, 84, and 180 ms prior to the hip impact, and activity at the time of hip impact averaged 72.3, 45.2, 64.3, and 63.4% of the peak activity. Furthermore, the outcome variables were associated with fall direction and/or knee position in all but the iliopsoas muscle. Conclusion: Our results provide insights on the hip muscle activation during a fall, which may help to understand the potential injury mechanism of the spontaneous hip fracture.

The two key variables of an Si solar cell, i.e., emitter (n-type window layer) and base (p-type substrate) doping levels or concentrations, are studied using Medici, a 2-dimensional semiconductor device simulation tool. The substrate is ptype and 150 μm thick, the pn junction is 2 μm from the front surface, and the cell is lit on the front surface. The doping concentration ranges from 1 × 1010 cm−3 to 1 × 1020 cm−3 for both emitter and base, resulting in a matrix of 11 by 11 or a total of 121 data points. With respect to increasing donor concentration (Nd) in the emitter, the open-circuit voltage (Voc) is little affected throughout, and the short-circuit current (Isc) is affected only at a very high levels of Nd, exceeding 1 × 1019 cm−3, dropping abruptly by about 12%, i.e., from Isc = 6.05 × 10−9 A·μm−1, at Nd = 1 × 1019 cm−3 to Isc = 5.35 × 10−9 A·μm−1 at Nd = 1 × 1020 cm−3, likely due to minority-carrier, or hole, recombination at the very high doping level. With respect to increasing acceptor concentration (Na) in the base, Isc is little affected throughout, but Voc increases steadily, i.e, from Voc = 0.29 V at Na = 1 × 1012 cm−3 to 0.69 V at Na = 1 × 1018 cm−3. On average, with an order increase in Na, Voc increases by about 0.07 V, likely due to narrowing of the depletion layer and lowering of the carrier recombination at the pn junction. At the maximum output power (Pmax), a peak value of 3.25 × 10−2 W· cm−2 or 32.5 mW· cm−2 is observed at the doping combination of Nd = 1 × 1019 cm−3, a level at which Si is degenerate (being metal-like), and Na = 1 × 1017 cm−3, and minimum values of near zero are observed at very low levels of Nd ≤ 1 × 1013 cm−3. This wide variation in Pmax, even within a given kind of solar cell, indicates that selecting an optimal combination of donor and acceptor doping concentrations is likely most important in solar cell engineering.

The effects of supplemental lighting (SL) timing on vegetative growth and the photosynthetic assimilation rate of young Cymbidium hybrids were examined. Nine month old C. ‘Yang Guifei’ and ‘Wine Shower’ were treated with four different SL timings: 22:00 – 02:00 (middle of the night, MN); 17:00 – 21:00 (end of day extension, DE); 07:00 – 09:00 plus 17:00 – 19:00 (both beginning and end of the night as split day extension, SDE), and non SL (8/16 h, short day, SD) for 4 months. All SL were provided by two types of 100% red LEDs (640 and 660 nm), with 150 μmol･m-2 ･s-1 and 800 μmol･mol-1 of CO2 supplied during the night (16 h). Pseudobulb diameters were significantly higher under SL treatments compared with the SD of both cultivars, irrespective of SL timing. Net photosynthetic assimilation rates were enhanced with increased SL, due to the additional photosynthesis and reduction of dark respiration. Thus, daily net photosynthetic amounts of SL treatments effectively increased photosynthesis compared to the SD. These results indicate that SL helps promote vegetative growth by enhancing photosynthesis. Since there were no significant differences among the SL timings when CO2 was provided uniformly during the night, we concluded that growth and photosynthesis of young Cymbidium do not depend on the timing of SL application, but are related to the daily light integrals, which is the amount of photosynthetically active photons delivered over 24 hours.

Runt related transcription factors (RUNX), a family of well-known transcription factors, play key regulatory roles in diverse biological processes, such as proliferation, differentiation, and DNA repair. Of RUNX family, RUNX3 is the least well characterized of the three family members. Nevertheless, the role of RUNX3 as a key regulator in essential biological pathways has been reported and inactivation of RUNX3 leads to a variety of disease, such as cancer, via regulation of Wnt signaling and K-ras mutations in many mammalian tissues. Recent studies using RUNX3-deficient cells and mice revealed an association with hematopoiesis and hypersensitivity to granulocytecolony stimulating factor. Nevertheless, protein dynamics associated with RUNX3 remain poorly understood. In the present study, we performed a large-scale protein study from Runx3 knockout (KO) mouse embryonic stem cells (mESC) using a stable isotope labeling by amino acids (SILAC)-based quantitative proteomics approach. The results showed that 67 proteins were significantly up and downregulated after Runx3 KO. Bioinformatic analyses that revealed that these proteins have diverse biological functions, such as substances transport and cellular structure. Thus, our results enhance our current understanding of the function of RUNX3 in mESCs and suggest potential roles for RUNX proteins in diverse diseases. Additionally, our results can be used as a database to help us understand the mechanism of action of RUNX3.

Tartary buckwheat has established itself as a functional food source because of its basic nutrition and phenolic compound contents, such as dietary fiber (DF) and rutin (RU). However, little information has been obtained concerning the comparative effects of DF and RU on the in vitro and in vivo glucose responses of tartary buckwheat flour. Moreover, the relationship between the flour’s in vitro starch digestibility and its components’ blood glucose response is not well-known. This study found that DF and RU reduced rapidly digestible starch (RDS) by 37.32→33.88% and 41.71→30.28%, whereas they increased resistant starch (RS) by 30.47→31.46% and 28.41→36.78%, respectively. Furthermore, RU had a lower glycemic index (GI) compared to DF. The regression equation for the in vitro and in vivo data from RU exhibited positive correlation (R 2 = 0.99); however, DF did not display positive correlation, which indicates that the in vitro and in vivo GI mechanisms by DF and RU are different.

We present an analysis of the chemical abundances and kinematics of six low-mass dwarf stars, previously claimed to be candidate hypervelocity stars (HVSs). We obtained moderate-resolution ($R\sim6000$) spectra of these stars to estimate the abundances of several chemical elements (Mg, Si, Ca, Ti, Cr, Fe, and Ni), and derived their space velocities and orbital parameters using proper motions from the \gaia\ Data Release 2. All six stars are shown to be bound to the Milky Way, and in fact are not even considered high-velocity stars with respect to the Galactic rest frame. Nevertheless, we attempt to characterize their parent Galactic stellar components by simultaneously comparing their element abundance patterns and orbital parameters with those expected from various Galactic stellar components. We find that two of our program stars are typical disk stars. For four stars, even though their kinematic probabilistic membership assignment suggests membership in the Galactic disk, based on their distinct orbit l properties and chemical characteristics, we cannot rule out exotic origins as follows. Two stars may be runaway stars from the Galactic disk. One star has possibly been accreted from a disrupted dwarf galaxy or dynamically heated from a birthplace in the Galactic bulge. The last object may be either a runaway disk star or has been dynamically heated. Spectroscopic follow-up observations with higher resolution for these curious objects will provide a better understanding of their origin.